{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:MUOKSBWXQ2ODRFAKTBGJXSSBJW","short_pith_number":"pith:MUOKSBWX","schema_version":"1.0","canonical_sha256":"651ca906d7869c38940a984c9bca414dba89bf6f856d9217ac8c6115aca93201","source":{"kind":"arxiv","id":"1112.1075","version":1},"attestation_state":"computed","paper":{"title":"Resolving multiple supermassive black hole binaries with pulsar timing arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alberto Sesana, Stanislav Babak","submitted_at":"2011-12-05T21:00:04Z","abstract_excerpt":"We study the capability of a pulsar timing array (PTA) to individually resolve and localize in the sky monochromatic gravitational wave (GW) sources. Given a cosmological population of inspiralling massive black hole binaries, their observable signal in the PTA domain is expected to be a superposition of several nearly-monochromatic GWs of different strength. In each frequency bin, the signal is neither a stochastic background nor perfectly resolvable in its individual components. In this context, it is crucial to explore how the information encoded in the spatial distribution of the array of "},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1112.1075","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-12-05T21:00:04Z","cross_cats_sorted":[],"title_canon_sha256":"07e802866d9ab1bc697b5429811b5587e4f82cca1bea0438c02b1ef365c1279e","abstract_canon_sha256":"5c59df55cd1f4f46c6c41df5fa756a8b50af21f299682cb1b18d988b039a6413"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:59:16.798708Z","signature_b64":"EJe4H4tqVfE8zmuV3vSofa7j8UAxtPleoH/BSCKbt3unxLAfzMx7dkymU10AQkvaO/DeP7fMWP90XDT1DXL6CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"651ca906d7869c38940a984c9bca414dba89bf6f856d9217ac8c6115aca93201","last_reissued_at":"2026-05-18T01:59:16.797926Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:59:16.797926Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Resolving multiple supermassive black hole binaries with pulsar timing arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alberto Sesana, Stanislav Babak","submitted_at":"2011-12-05T21:00:04Z","abstract_excerpt":"We study the capability of a pulsar timing array (PTA) to individually resolve and localize in the sky monochromatic gravitational wave (GW) sources. Given a cosmological population of inspiralling massive black hole binaries, their observable signal in the PTA domain is expected to be a superposition of several nearly-monochromatic GWs of different strength. In each frequency bin, the signal is neither a stochastic background nor perfectly resolvable in its individual components. In this context, it is crucial to explore how the information encoded in the spatial distribution of the array of "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1112.1075","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1112.1075","created_at":"2026-05-18T01:59:16.798065+00:00"},{"alias_kind":"arxiv_version","alias_value":"1112.1075v1","created_at":"2026-05-18T01:59:16.798065+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1112.1075","created_at":"2026-05-18T01:59:16.798065+00:00"},{"alias_kind":"pith_short_12","alias_value":"MUOKSBWXQ2OD","created_at":"2026-05-18T12:26:37.096874+00:00"},{"alias_kind":"pith_short_16","alias_value":"MUOKSBWXQ2ODRFAK","created_at":"2026-05-18T12:26:37.096874+00:00"},{"alias_kind":"pith_short_8","alias_value":"MUOKSBWX","created_at":"2026-05-18T12:26:37.096874+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.28571","citing_title":"The NANOGrav 15 yr Data Set: Customized Chromatic Noise Models","ref_index":140,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28554","citing_title":"The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave Analyses","ref_index":130,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW","json":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW.json","graph_json":"https://pith.science/api/pith-number/MUOKSBWXQ2ODRFAKTBGJXSSBJW/graph.json","events_json":"https://pith.science/api/pith-number/MUOKSBWXQ2ODRFAKTBGJXSSBJW/events.json","paper":"https://pith.science/paper/MUOKSBWX"},"agent_actions":{"view_html":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW","download_json":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW.json","view_paper":"https://pith.science/paper/MUOKSBWX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1112.1075&json=true","fetch_graph":"https://pith.science/api/pith-number/MUOKSBWXQ2ODRFAKTBGJXSSBJW/graph.json","fetch_events":"https://pith.science/api/pith-number/MUOKSBWXQ2ODRFAKTBGJXSSBJW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW/action/storage_attestation","attest_author":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW/action/author_attestation","sign_citation":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW/action/citation_signature","submit_replication":"https://pith.science/pith/MUOKSBWXQ2ODRFAKTBGJXSSBJW/action/replication_record"}},"created_at":"2026-05-18T01:59:16.798065+00:00","updated_at":"2026-05-18T01:59:16.798065+00:00"}